Cosmic Ray Energy Determination by the Reduced-Opening Angle Method

Details Cosmic Ray Energy Determination by the Reduced-Opening Angle Method Cosmic Ray Energy Determination by the Reduced-Opening Angle Method

Feb 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998nasa.reptu....s&link_type=abstract

Technical Report, NASA/CR-1998-207914; NAS 1.26:207914 Cosmic Ray Lab.

Mathematics

Logic

Cosmic Rays, Radiation Measurement, Galactic Cosmic Rays, Silicon, Protons, Phenomenology, Iron, Enrichment, Deployment

Scientific paper

Accurate measurement of the primary galactic cosmic ray species energy dependence in the regime beyond approx. 500 GeV/a is difficult due to the low flux and the limitations of energy measurement techniques. However, such observations are essential to resolve several questions of current interest such as: Is the enrichment of heavy species (Z greater that or equal to 6) cosmic rays first reported at higher energies by the proton satellite' and then later at lower energies real? The results from a previous deployment of the reduced opening angle technique are inconclusive but the authors do point to limitations in the previous techniques. Another intriguing puzzle is the energy dependence of silicon cosmic rays. Two independent experiments using different experimental techniques indicate that silicon is under-abundant. At present the observation is limited by statistics; it could still be a three sigma fluctuation. However, if confirmed the current models of acceleration and propagation which are species independent are seriously inadequate. To progress further the species and energy dependence must be accurately measured in a manner that is free from systematic uncertainty. In this report we show that the reduced opening angle method offers a simple and relatively inexpensive method to answer these questions. First we present the physics of the reduced opening angle and indicate the expected energy and charge resolution. The proposed detector design is then presented followed by the expected performance. Where ever possible simple phenomenological expressions that allow 'back of the envelope' estimates are given. More details are presented in the appendices. The limit of the energy resolution and the expected event rates for iron cosmic rays are calculated. Salient points are summarized in the conclusions.

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